Supernovae (SNe) are believed to be the dominant sources of dust production at high redshift. However, the reverse shock generated by the interaction of the SN forward shock and the interstellar medium (ISM) can significantly reduce the mass of newly formed dust in SN ejecta. This study quantifies the mass, composition, and grain size distribution of surviving dust after the passage of the reverse shock using the GRASHrev model. Our analysis covers a grid of SN models with progenitor masses 13M_{sun}<=m_star<=120M_{sun}, metallicity -3=10nm) are more resistant to destruction by the reverse shock, with amorphous carbon dominating the surviving dust mass in most models. The surviving dust mass decreases with increasing ISM density. For non-rotating progenitors, the maximum mass of dust surviving the passage of the reverse shock is ~0.02M{sun} released by SN explosions of a 120 Msun progenitor with [Fe/H]=0 in the ISM density 0.5cm^-3^, corresponding to ~4% of the initial dust mass before the passage of the reverse shock. Similarly, among the rotating progenitors, a maximum surviving mass fraction is ~5% with a final dust mass ~0.03M{sun}_ in [Fe/H]=-1 models. Although the reverse shock has a strong destructive impact, our results indicate that, on very short timescales of 6, suggesting the early presence of such dust.