1992; Kumai, Basu, & Fujimoto 1993a). Alternatively, additional globulars might be captured by a large galaxy that accretes small, gas-poor systems (e.g., Côté et al. 1998) or accumulates tidal debris from other members in a cluster of galaxies (see Muzzio 1987). However, processes such as these also increase the total masses of gas and/or stars in the final system. In [*large*]{} galaxies (i.e., in those that do not suffer significant gas loss from strong galactic winds; cf. §4.2), any changes in the ratio $M_{\rm
gcs}/(M_{\rm gas}+M_{\rm stars})$ are bound to be smaller than changes in either of these quantities individually. The presently observed ${\hbox{$\widehat\epsilon$}}_
{\rm cl}$ in any large galaxy with a complex dynamical history is then a mass-weighted average of the true $\epsilon_{\rm cl}$ in some number of discrete star-formation events and individual accreted systems; and in the limit that the underlying efficiency of cluster formation is independent of environment and epoch (as the results of §§3 and 4 will suggest is nearly correct), it is still true that ${\hbox{$\widehat\epsilon$}}_{\rm cl}\simeq\epsilon_{\rm
cl}$—just as in the case of passive evolution, and subject only to the small error associated there with the effects of GCS erosion by cluster evaporation and tidal 