I am going to start with this paragraph from Wikipedia (emphasis mine):

The most important fusion process in nature is the one that powers
stars. In the 20th century, it was realized that the energy released
from nuclear fusion reactions accounted for the longevity of the Sun
and other stars as a source of heat and light. The fusion of nuclei in
a star, starting from its initial hydrogen and helium abundance,
provides that energy and synthesizes new nuclei as a byproduct of that
fusion process. The prime energy producer in the Sun is the fusion of
hydrogen to form helium, which occurs at a solar-core temperature of
14 million kelvin. The net result is the fusion of four protons into
one alpha particle, with the release of two positrons, two neutrinos
(which changes two of the protons into neutrons), and energy.
Different reaction chains are involved, depending on the mass of the
star. For stars the size of the sun or smaller, the proton-proton
chain dominates. In heavier stars, the CNO cycle is more important.

The proton-proton chain set of reactions look like this:

The CNO cycle looks like this:

Net Result

Either way, the net result is 4 protons ($^1\!$H nuclei) are turned into 1 alpha particle ($^4\!$He nucleus) plus 2 positrons (e$^+$). The 2 positrons go on to annihilate 2 electrons, so altogether we have a mass change of $$ \Delta M = M_{\mathsf \alpha} - 2M_{\mathsf e} - 4M_{\mathsf P}\,. $$

Let's find out the fractional change in mass: $$ f_\Delta = \frac{\Delta M}{4M_{\mathsf P}} = \frac{M_{\mathsf \alpha} - 2M_{\mathsf e} - 4M_{\mathsf P}}{4M_{\mathsf P}}\,. $$

Now the ratio of the mass of an alpha particle to a proton is $3.9726$, or $$ M_{\mathsf \alpha} = 3.9726\times M_{\mathsf P}\,. $$

The ratio of the mass of a proton to an electron is $1836.1$, or $$ M_{\mathsf e} = \frac{M_{\mathsf P}}{1836.1} = 0.0005446\times M_{\mathsf P}\,. $$

Substituting into the $f_\Delta$ equation, $$ f_\Delta = \frac{3.9726\times M_{\mathsf P} - 0.0011\times M_{\mathsf P} - 4\times M_{\mathsf P}}{4\times M_{\mathsf P}} = \frac{-0.0285}4 = -0.007125 = -0.7125\%\,\,.$$

So obviously, Even if all of the hydrogen were converted (only a fraction actually is) the loss of mass to the star would be too negligible to matter.

A more important mass loss for large stars is that from their stellar wind, which for very large main sequence stars (types O or B) removes a sizable fraction of the very large star's mass over it's lifetime.