Notes. Column (2) lists disk dissipation studies where the clusters in Col. (1) were included. The numbers in Cols. (3) and (4) are based on such studies and references therein. The age range is indicated in Col. (3). Following Mamajek (2009), an uncertainty of 30% has been assigned to ages without error bars. Column (4) indicates whether the cluster has a total stellar mass above or below 500−1000 M_⊙ (yes or no), which is in turn indicative of the presence of a significant number of massive OB stars within the clusters (but we note that most are part of OB associations when larger scales are considered; see, e.g., Wright 2020). The presence or absence of evidence indicating cluster expansion (yes or no) is indicated in Col. (5) whenever available in Kuhn et al. (2019). The last three columns are based on our work. The average Gaia EDR3 distance (and standard deviation) to each cluster is shown in Col. (6) (see Appendix C). Columns (7) and (8) show the surface density of member stars for the inner FOV_2 pc and the whole FOV_20 pc, as inferred from Table A.1.

References. ⁽¹⁾Hernández et al. (2008), ⁽²⁾Mamajek (2009), ⁽³⁾Muzerolle et al. (2010), ⁽⁴⁾Pfalzner et al. (2014), ⁽⁵⁾Ribas et al. (2015), ⁽⁶⁾Guarcello et al. (2021), ⁽⁷⁾Haisch et al. (2001), ⁽⁸⁾Fedele et al. (2010). ^( † 1)Panja et al. (2021), ^( † 2)Wang et al. (2011), ^( † 3)Saurin et al. (2012).