  We use a high resolution collisionless simulation of a Virgo--like cluster in
a $\Lambda$CDM cosmology to determine the velocity and clustering properties of
the diffuse stellar component in the intracluster region at the present epoch.
The simulated cluster builds up hierarchically and tidal interactions between
member galaxies and the cluster potential produce a diffuse stellar component
free-flying in the intracluster medium. Here we adopt an empirical scheme to
identify tracers of the stellar component in the simulation and hence study its
properties. We find that at $z=0$ the intracluster stellar light is mostly
unrelaxed in velocity space and clustered in structures whose typical
clustering radii are about 50 kpc at R=400--500 kpc from the cluster center,
and predict the radial velocity distribution expected in spectroscopic
follow-up surveys. Finally, we compare the spatial clustering in the simulation
with the properties of the Virgo intracluster stellar population, as traced by
ongoing intracluster planetary nebulae surveys in Virgo. The preliminary
results indicate a substantial agreement with the observed clustering
properties of the diffuse stellar population in Virgo.
