  Stars form within dense cores composed of both gas and dust within molecular
clouds. However, despite the crucial role that dust plays in the star formation
process, its dynamics is frequently overlooked, with the common assumption
being a constant, spatially uniform dust-to-gas ratio and grain size spectrum.
In this study, we introduce a set of radiation-dust-magnetohydrodynamic
simulations of star forming molecular clouds from the {\small STARFORGE}
project. These simulations expand upon the earlier radiation MHD models, which
included cooling, individual star formation, and feedback. Notably, they
explicitly address the dynamics of dust grains, considering radiation, drag,
and Lorentz forces acting on a diverse size spectrum of live dust grains. We
find that interactions between radiation and dust significantly influence the
properties of gas surrounding and accreting onto massive stars. Specifically,
we find that once stars exceed a certain mass threshold ($\sim 2 M_{\odot}$),
their emitted radiation can evacuate dust grains from their vicinity, giving
rise to a dust-suppressed zone of size $\sim 100$ AU. Commencing during the
early accretion stages and preceding the Main-sequence phase, this process
results in a mass-dependent depletion in the accreted dust-to-gas (ADG) mass
ratio within both the circumstellar disc and the star. We predict massive stars
($\gtrsim 10 M_{\odot}$) would exhibit ADG ratios that are approximately one
order of magnitude lower than that of their parent clouds. Consequently, stars,
their discs, and circumstellar environments would display notable deviations in
the abundances of elements commonly associated with dust grains, such as carbon
and oxygen.
