Estimated probability density function values of binned star cluster masses in disk- (B/T < 0.2; blue colour) and bulge-dominated (B/T > 0.7; red colour) galaxies at z = 0. We track up to 2000 star clusters per galaxy, split equally between star clusters located in the disk (top row) and halo (bottom row). Host galaxies are separated into three mass bins. Additionally, we separate between young (τ_c ≤ 300 Myr; solid lines) and old (τ_c > 6 Gyr; shaded regions) star clusters. We sample the CIMF with an initial mass of 10⁴ M_⊙ and discard star clusters with masses below 10³ M_⊙. The black solid line in the top left panel presents the asymptotic power-law behaviour towards m_c = 0. We compare the population of simulated star clusters to the observational resulted of Brown & Gnedin (2021, orange colour). Each column shows the same dataset as the location of the star clusters (disk versus halo) is not specified by the authors.