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 tantalizing features by comparing constrained LG and field central dwarf halo simulations in the NIHAO project. For the first time, constrained LG simulations performed with NIHAO hydrodynamics which track the evolution of MW and M31 along with ~100 dwarfs in the Local Group are presented. The total gas mass and stellar properties (velocity dispersion, evolution history, etc.) of present-day LG dwarfs are found to be similar to field systems. Overall, the simulated LG dwarfs show representative stellar properties to other dwarfs in the Universe. However, relative to fields, LG dwarfs have more cold gas in their central parts and more metal-rich gas in the halo stemming from interactions with MW/M31 and/or feedback. The larger gas metal content in LG dwarfs results in early star formation events that lead to strong feedback and subsequent quenching. We also test for the impact of metal diffusion on the chemical evolution of LG dwarfs, and find that metal diffusion does not affect the stellar or gaseous content of LG relative to field dwarfs; the largest differences are found with the gas metallicity (~0.1 dex). Our results show that properties from LG dwarfs may be used as general constraints for studying the overall dwarf population in the Universe, providing a powerful local laboratory for galaxy formation tests and comparisons.
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