  We implement a state-of-the-art treatment of the processes affecting the
production and Interstellar Medium (ISM) evolution of carbonaceous and silicate
dust grains within SPH simulations. We trace the dust grain size distribution
by means of a two-size approximation. We test our method on zoom-in simulations
of four massive ($M_{200} \geq 3 \times 10^{14} M_{\odot}$) galaxy clusters. We
predict that during the early stages of assembly of the cluster at $z \gtrsim
3$, where the star formation activity is at its maximum in our simulations, the
proto-cluster regions are rich of dusty gas. Compared to the case in which only
dust production in stellar ejecta is active, if we include processes occurring
in the cold ISM,the dust content is enhanced by a factor $2-3$. However, the
dust properties in this stage turn out to be significantly different than those
observationally derived for the {\it average} Milky Way dust, and commonly
adopted in calculations of dust reprocessing. We show that these differences
may have a strong impact on the predicted spectral energy distributions. At low
redshift in star forming regions our model reproduces reasonably well the trend
of dust abundances over metallicity as observed in local galaxies. However we
under-produce by a factor of 2 to 3 the total dust content of clusters
estimated observationally at low redshift, $z \lesssim 0.5$ using IRAS, Planck
and Herschel satellites data. This discrepancy can be solved by decreasing the
efficiency of sputtering which erodes dust grains in the hot Intracluster
Medium (ICM).
