provided by the Padova group [@marigo2008] (version 2.3) and obtained via the online server CMD[^4].

We did not find a visual correlation between separation from H[ii]{} regions and colours of star clusters for objects with SC-H[ii]{}R deprojected separation larger than 8 arcsec.

@efremov1998 estimated a duration of star formation in star complexes at large spatial scales (500-1000 pc) to be about 30 Myr. Among star clusters within a complex, both very young ($<10$ Myr) and intermediate-age objects ($\sim100$ Myr) are encountered. The colour indices of star clusters in Fig. \[figure:ubv\_sep\] correspond to the range from several Myr to a few hundred Myr (see Fig. \[figure:ubv\_age\]).

Our angular resolution does not allow us to study stellar groups at the scale of star clusters in distant galaxies. For larger star formation regions, SSP model is not correct [@efremov1998] and the colours of these stellar groups depend on both the age and the star formation history. For this reason we eliminated three distant ($D>$ 20 Mpc) galaxies NGC 266, NGC 2336, and NGC 6217 from further consideration. We also excluded the high inclination galaxy NGC 7331 ($i=75\degr$), because of large uncertainty of projection effects.

The sample of remaining five galaxies is presented in 