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More and more observations indicate that young star clusters could retainimprints of their formation process. In particular, the degree ofsubstructuring and rotation are possibly the direct result of the collapse ofthe parent molecular cloud from which these systems form. Such properties can,in principle, be washed-out, but they are also expected to have an impact onthe relaxation of these systems. We ran and analyzed a set of tenhydrodynamical simulations of the formation of embedded star clusters throughthe collapse of turbulent massive molecular clouds. We systematically studiedthe fractality of our star clusters, showing that they are all extremelysubstructured (fractal dimension $D=1.0-1.8$). We also found that fractality isslowly reduced, with time, on small scales, while it persists on large scaleson longer timescales. Signatures of rotation are found in different simulationsat every time of the evolution, even for slightly supervirial substructures,proving that the parent molecular gas transfers part of its angular momentum tothe new stellar systems.

Evolution of fractality and rotation in embedded star clusters