CMDs of the candidate intermediate-age clusters (stars selected in the same annuli as in Figs. 4 and 5) before (left panels) and after (right panels) the statistical decontamination from field stars. We superposed on the CMDs the youngest-age isochrones whose upper MS and SGB trace the blue/bright edge of the observed stars to set a strong lower limit to the age of the clusters (metallicity, reddening, and distances are the same as those adopted in Figs. 4 and 5). The age of the adopted isochrone is reported as a label in the upper-right corner of the left panels. Note, however, that there are no such faint stars in the de-contaminated CMD, suggesting that they are not associated to the clusters.