  The post-reionization ${\rm HI}$ 21-cm signal is an excellent candidate for
precision cosmology, this however requires accurate modelling of the expected
signal. Sarkar et al. (2016) have simulated the real space ${\rm HI}$ 21-cm
signal, and have modelled the ${\rm HI}$ power spectrum as $P_{{\rm HI}}(k)=b^2
P(k)$ where $P(k)$ is the dark matter power spectrum and $b(k)$ is a (possibly
complex) scale dependent bias for which fitting formulas have been provided.
This paper extends these simulations to incorporate redshift space distortion
and predict the expected redshift space ${\rm HI}$ 21-cm power spectrum
$P^s_{{\rm HI}}(k_{\perp},k_{\parallel})$ using two different prescriptions for
the ${\rm HI}$ distributions and peculiar velocities. We model $P^s_{{\rm
HI}}(k_{\perp},k_{\parallel})$ assuming that it is the product of $P_{{\rm
HI}}(k)=b^2 P(k)$ with a Kaiser enhancement term and a Finger of God (FoG)
damping which has $\sigma_p$ the pair velocity dispersion as a free parameter.
Considering several possibilities for the bias and the damping profile, we find
that the models with a scale dependent bias and a Lorentzian damping profile
best fit the simulated $P^s_{{\rm HI}}(k_{\perp},k_{\parallel})$ over the
entire range $1 \le z \le 6$. The best fit value of $\sigma_p$ falls
approximately as $(1+z)^{-m}$ with $m=2$ and $1.2$ respectively for the two
different prescriptions. The model predictions are consistent with the
simulations for $k < 0.3 \, {\rm Mpc}^{-1}$ over the entire $z$ range for the
monopole $P^s_0(k)$, and at $z \le 3$ for the quadrupole $P^s_2(k)$. At $z \ge
4$ the models underpredict $P^s_2(k)$ at large $k$, and the fit is restricted
to $k < 0.15 \, {\rm Mpc}^{-1}$.
