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In this paper, we discuss the origin of the observed correlation betweencluster concentration c and present-day mass function (PDMF) slope {\alpha}reported by De Marchi, Paresce & Pulone. This relation can either be reproducedfrom universal initial conditions combined with some dynamical mechanism(s)that alter(s) the cluster structure and mass function over time, or it mustarise early on in the cluster lifetime, such as during the gas-embedded phaseof cluster formation. Using a combination of Monte Carlo and N-body models forglobular cluster evolution performed with the MOCCA and NBODY6 codes,respectively, we explore a number of dynamical mechanisms that could affect theobserved relation.  For the range of initial conditions considered here, our results areconsistent with an universal initial binary fraction \approx 10% (which doesnot, however, preclude 100%) and an universal initial stellar mass functionresembling the standard Kroupa distribution. Most of the dispersion observed inthe c-{\alpha} relation can be attributed to two-body relaxation and Galactictides. However, dynamical processes alone could not have reproduced thedispersion in concentration, and we require at least some correlation betweenthe initial concentration and the total cluster mass. We argue that the originof this trend could be connected to the gas-embedded phase of clusterevolution.

The state of globular clusters at birth: emergence from the gas-embedded phase