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In this paper we discuss the cluster and field star formation in the centralpart of the Small Magellanic Cloud. The main goal is to study the correlationbetween young objects and their interstellar environment. The ages of about 164associations and 311 clusters younger than 1 Gyr are determined using isochronefitting. The spatial distribution of the clusters is compared with the HI maps,with the HI velocity dispersion field, with the location of the CO clouds andwith the distribution of young field stars. The cluster age distributionsupports the idea that clusters formed in the last 1 Gyr of the SMC history ina roughly continuous way with periods of enhancements. The two super-shells 37Aand 304A detected in the HI distribution are clearly visible in the agedistribution of the clusters: an enhancement in the cluster formation rate hastaken place from the epoch of the shell formation. A tight correlation betweenyoung clusters and the HI intensity is found. The degree of correlation isdecreasing with the age of the clusters. Clusters older than 300 Myr arelocated away from the HI peaks. Clusters and associations younger than 10 Myrare related to the CO clouds in the SW region of the SMC disk. A positivecorrelation between the location of the young clusters and the velocitydispersion field of the atomic gas is derived only for the shell 304A,suggesting that the cloud-cloud collision is probably not the most importantmechanism of cluster formation. Evidence of gravitational triggered episode dueto the most recent close interaction between SMC and LMC is found both in thecluster and field star distribution.

Age distribution of young clusters and field stars in the Small Magellanic Cloud