  Stars and their corresponding protoplanetary disks form in diverse
environments. To account for these natural variations, we investigate the
formation process around nine solar mass stars with a maximum resolution of 2
AU in a Giant Molecular Cloud of (40 pc)$^3$ in volume by using the adaptive
mesh refinement code \ramses. The magnetohydrodynamic simulations reveal that
the accretion process is heterogeneous in time, in space, and among protostars
of otherwise similar mass. During the first roughly 100 kyr of a protostar
evolving to about a solar mass, the accretion rates peak around $10^{-5}$ to
$10^{-4}$ M$_{\odot}$ yr$^{-1}$ shortly after its birth, declining with time
after that. The different environments also affect the spatial accretion, and
infall of material to the star-disk system is mostly through filaments and
sheets. Furthermore, the formation and evolution of disks varies significantly
from star to star. We interpret the variety in disk formation as a consequence
of the differences in the combined effects of magnetic fields and turbulence
that may cause differences in the efficiency of magnetic braking, as well as
differences in the strength and distribution of specific angular momentum.
