  We are entering an era in which we will be able to detect and characterize
hundreds of dwarf galaxies within the Local Volume. It is already known that a
strong dichotomy exists in the gas content and star formation properties of
field dwarf galaxies versus satellite dwarfs of larger galaxies. In this work,
we study the more subtle differences that may be detectable in galaxies as a
function of distance from a massive galaxy, such as the Milky Way. We compare
smoothed particle hydrodynamic simulations of dwarf galaxies formed in a Local
Volume-like environment (several Mpc away from a massive galaxy) to those
formed nearer to Milky Way-mass halos. We find that the impact of environment
on dwarf galaxies extends even beyond the immediate region surrounding Milky
Way-mass halos. Even before being accreted as satellites, dwarf galaxies near a
Milky Way-mass halo tend to have higher stellar masses for their halo mass than
more isolated galaxies. Dwarf galaxies in high-density environments also tend
to grow faster and form their stars earlier. We show observational predictions
that demonstrate how these trends manifest in lower quenching rates, higher HI
fractions, and bluer colors for more isolated dwarf galaxies.
