Stacked analyses of galaxy clusters at low-to-intermediate redshift show signatures attributable to dust, but the origin of this dust is uncertain. I will first give an overview of known dust properties, then I will introduce approaches to dust evolution modeling. I applied our models to two contexts: (1) zoom-in cosmological simulations of massive galaxy clusters (10^14 to 10^15 solar masses) and (2) reconstructions of typical galaxy clusters through integrating one-zone evolutions of elliptical, spiral, and irregular galaxies over luminosity functions. In both cases, the scant dust abundances in the intracluster medium are attributable either to dust recently ejected from spiral galaxies or to unresolved cold/active objects. The total dust-to-gas mass ratio in galaxy clusters amounts to 10^−4, while the intracluster medium dust-to-gas mass ratio amounts to 10^−6 at most. These dust abundances are consistent with the estimates of cluster observations at 0.2 < z < 1.