  {It is necessary to understand the dynamics of the atomic gas to use complex
modeling and to carry out detailed comparisons between theoretical models and
observations.}{In a companion paper, we present high resolution bidimensional
numerical simulations of the interstellar atomic hydrogen. Here, we further
characterize these simulations and we compare our results with various
observations.}{We give statistics of the column density and velocity along the
line of sight and show that they compare favorably with observations of
high-latitude lines of sight. We compute synthetic HI spectra and qualitatively
discuss the information that could be inferred if these spectra were observed.
Finally, we extract CNM clouds and study their physical properties finding
strong similarities with real clouds. In particular, we find that the clouds
follow Larson-type relations, i.e. $M \propto L^\gamma$, where $\gamma \simeq
1.7$ (we speculate that in 3D, $\gamma \simeq 2.5$) and $\sqrt{<\delta v^2>}
\propto L^{0.4}$. We also find that the distribution, ${\cal N}(N)$, of the
column density, $N$, of the CNM structures formed in the simulation follows
${\cal N}(N) \propto N^{-1.2}$ which is marginally compatible with the
observational result obtained by Heiles & Troland (2005). From the mass-size
relation and the mass spectrum, we derive an exponent for the column density
distribution close to the value obtained in the numerical simulation.} {We
conclude that the simulations reproduce various observational features
reasonably well....}
