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