  We combine high resolution N-body simulations with deep observations of
neutral hydrogen (HI) in nearby galaxy groups in order to explore two
well-known theories of HI cloud formation: HI stripping by galaxy interactions
and dark matter minihalos with embedded HI gas. This paper presents new data
from three galaxy groups, Canes Venatici I, NGC 672, and NGC 45, and assembles
data from our previous galaxy group campaign to generate a rich HI cloud
archive to compare to our simulated data.
  We find no HI clouds in the Canes Venatici I, NGC 672, or NGC 45 galaxy
groups. We conclude that HI clouds in our detection space are most likely to be
generated through recent, strong galaxy interactions. We find no evidence of HI
clouds associated with dark matter halos above M_HI = 10^6 M_Sun, within +/-
700 km/s of galaxies, and within 50 kpc projected distance of galaxies.
