  I review the properties of the interstellar medium in the Magellanic Clouds
and Local Group dwarf galaxies. The more massive, star-forming galaxies show a
complex, multi-phase ISM full of shells and holes ranging from very cold phases
(a few 10 K) to extremely hot gas (> 10^6 K). In environments with high UV
radiation fields the formation of molecular gas is suppressed, while in dwarfs
with low UV fields molecular gas can form at lower than typical Galactic column
densities. There is evidence of ongoing interactions, gas accretion, and
stripping of gas in the Local Group dwarfs. Some dwarf galaxies appear to be in
various stages of transition from gas-rich to gas-poor systems. No ISM was
found in the least massive dwarfs.
