  Measuring the distribution of stellar spin axis orientations in a coeval
group of stars probes the physical processes underlying the stars' formation.
In this paper, we use spectro-photometric observations of the open cluster NGC
2516 to determine the degree of spin alignment among its stars. We combine TESS
light curves, ground-based spectroscopy from the Gaia-ESO and GALAH surveys,
broad-band stellar magnitudes from several surveys, and Gaia astrometry to
measure 33 stellar inclinations and quantify overall cluster rotation. Our
measurements suggest that stellar spins in this cluster are isotropically
oriented, while allowing for the possibility that they are moderately aligned.
An isotropic distribution of NGC 2516 spins would imply a star-forming
environment in which turbulence dominated ordered motion, while a moderately
aligned distribution would suggest a more substantial contribution from
rotation. We also perform a three-dimensional analysis of the cluster's
internal kinematics, finding no significant signatures of overall rotation.
Stemming from this analysis, we identify evidence of cluster contraction,
suggesting possible ongoing mass segregation in NGC 2516.
