  Recent studies have identified star clusters with multiple components based
on accurate spatial distributions and/or proper motions from Gaia DR3,
utilising diverse diagnostics to improve our understanding of subgroup
evolution. These findings motivated us to search for subgroups among the
objects examined in our previous work, which employed fractal statistics. The
present study considers seven open clusters that exhibit significant dispersion
in age and/or proper motion distributions, suggesting that they would not be
single clusters. For characterizing the stellar groups, we calculate the
membership probability using Bayesian multi-dimensional analysis by fitting the
observed proper motion distribution of the candidates. A probability
distribution is also used to determine the distance of the cluster, which is
obtained from the mean value of the distance modes. The photometry from Gaia
DR3 is compared with evolutionary models to estimate the cluster age and total
mass. In our sample, double components are found only for Markarian 38 and NGC
2659. The other five clusters are confirmed as being single. The structural
parameters, such as Q, Lambda_MSR and Sigma_LDR are compared with results from
N-body simulations to investigate how the morphology of the stellar clustering
evolves. The new results, for a more complete sample of cluster members,
provide a better definition of the distribution type (central concentration or
substructured region) inferred from the m-s plot.
