  Recent observational and theoretical studies of the Local Group (LG) dwarf
galaxies have highlighted their unique star-formation history, stellar
metallicity, gas content, and kinematics. We investigate the commonality of
these features by comparing constrained LG and field central dwarf halo
simulations in the Numerical Investigation of a Hundred Astrophysical Objects
(NIHAO) project. Our simulations, performed with NIHAO-like hydrodynamics which
track the evolution of the Milky Way (MW) and M31 along with ~100 dwarfs in the
LG, reveal the total gas mass and stellar properties (velocity dispersion,
evolution history, etc.) of present-day LG dwarfs to be similar to field
systems. However, relative to field galaxies, LG dwarfs have more cold gas in
their central parts and more metal-rich gas in the halo stemming from
interactions with other dwarfs living in a high-density environment like the
LG. Interestingly, the direct impact of massive MW/M31 analogues on the
metallicity evolution of LG dwarfs is minimal; LG dwarfs accrete
high-metallicity gas mostly from other dwarfs at late times. We have also
tested for the impact of metal diffusion on the chemical evolution of LG
dwarfs, and found that it does not affect the stellar or gaseous content of LG
dwarfs. Our simulations suggest that the stellar components of LG dwarfs offer
a unique and unbiased local laboratory for galaxy-formation tests and
comparisons, especially against the overall dwarf population in the Universe.
