  Using a cosmological dark matter simulation of a galaxy-cluster halo, we
follow the temporal evolution of its globular cluster population. To mimic the
red and blue globular cluster populations, we select at high redshift $(z\sim
1)$ two sets of particles from individual galactic halos constrained by the
fact that, at redshift $z=0$, they have density profiles similar to observed
ones. At redshift $z=0$, approximately 60\% of our selected globular clusters
were removed from their original halos building up the intra-cluster globular
cluster population, while the remaining 40\% are still gravitationally bound to
their original galactic halos. Since the blue population is more extended than
the red one, the intra-cluster globular cluster population is dominated by blue
globular clusters, with a relative fraction that grows from 60\% at redshift
$z=0$ up to 83\% for redshift $z\sim 2$. In agreement with observational
results for the Virgo galaxy cluster, the blue intra-cluster globular cluster
population is more spatially extended than the red one, pointing to a tidally
disrupted origin.
