Left panel: fraction of cluster Cepheids p_CC(M_ecl) (including UpCeps) as a function of cluster mass M_ecl integrated over the first 300 Myr of the cluster evolution. Clusters orbiting at different galactocentric radii R_g are denoted by different symbols; clusters with different metallicity Z are denoted by different colour of the symbol. The external field of the galaxy, which impacts the lower mass clusters more, is responsible for the decrease of p_CC(M_ecl) with R_g. p_CC(M_ecl) increases with M_ecl because more massive clusters withstand gas expulsion and the tidal field of the galaxy better. For lower mass clusters, p_CC(M_ecl) decreases with metallicity because Cepheids occur later at lower Z, at which time more low-mass clusters have been dissolved. Right panel: mean mass of Cepheids in the cluster as a function of M_ecl. At a given metallicity, peaks at a cluster mass of 200 M_⊙ because lower mass clusters do not live long enough to host lower mass Cepheids. The decrease of with decreasing Z is caused by the decreasing lower mass limit m_min, Ceph for Cepheids with Z.