  This is the second paper in a series presenting the results from a 500
$h^{-1}$Mpc large constrained hydro-dynamical simulation of the local Universe
(SLOW). The initial conditions are based on peculiar velocities derived from
the CosmicFlows-2 catalogue. The inclusion of galaxy formation treatment,
allows to directly predict observable properties of the Intra-Cluster Medium
(ICM) within galaxy clusters. Comparing the properties of observed galaxy
clusters within the local Universe with the properties of their simulated
counterparts, enables us to assess the effectiveness of the initial condition
constraints in accurately replicating the non-linear properties of the largest,
collapsed objects within the simulation. Based on the combination of several,
publicly available surveys, we identified 45 local Universe galaxy clusters in
SLOW, including the 13 most massive from the Planck SZ catalog and 70% of those
with $M_{500} > 2\times 10^{14}$ M$_{\odot}$. We then derived the probability
of the cross identification based on mass, X-ray luminosity, temperature and
Compton-y by comparing it to a random selection. In relation to previous
constrained simulations of the local volume, we found in SLOW a much larger
amount of replicated galaxy clusters, where their simulation based mass
prediction falls within the uncertainties of the observational mass estimates.
Comparing the median observed and simulated masses of our cross identified
sample allows to independently deduce a hydrostatic mass bias of
$(1-b)\approx0.87$. The SLOW constrained simulation of the local Universe
faithfully reproduces numerous fundamental characteristics of the galaxy
clusters within our local neighbourhood, opening a new avenue for studying the
formation and evolution of a large set of individual galaxy clusters as well as
testing our understanding of physical processes governing the ICM.
