  The current kinematic state of young stellar clusters can give clues on their
actual dynamical state and origin. In this contribution, we use Gaia DR3 data
of the Lagoon Nebula Cluster (LNC) to show that the cluster is composed of two
expanding groups, likely formed from different molecular cloud clumps. We find
no evidence of massive stars having larger velocity dispersion than low-mass
stars or being spatially segregated across the LNC, as a whole, or within the
Primary group. However, the Secondary group, with 1/5th of the stars, exhibits
intriguing features. On the one hand, it shows a bipolar nature, with an aspect
ratio of $\sim$3:1. In addition, the massive stars in this group exhibit larger
velocity dispersion than the low-mass stars, although they are not concentrated
towards the center of the group. This suggests that this group may have
undergone dynamical relaxation, first, and some explosive event afterward.
However, further observations and numerical work have to be performed to
confirm this hypothesis. The results of this work suggest that, although
stellar clusters may form by the global and hierarchical collapse of their
parent clump, still some dynamical relaxation may take place.
