We investigate the origin of the shape of the globular cluster ( GC ) system scaling parameters as a function of galaxy mass , i.e . specific frequency ( S _ { N } ) , specific luminosity ( S _ { L } ) , specific mass ( S _ { M } ) , and specific number ( \hat { T } ) of GCs . In the low-mass galaxy regime ( M _ { V } \ga -16 mag ) our analysis is based on HST/ACS observations of GC populations of faint , mainly late-type dwarf galaxies in low-density environments . In order to sample the entire range in galaxy mass ( M _ { V } = -11 to -23 mag = 10 ^ { 6 } - 10 ^ { 11 } L _ { \odot } ) , environment , and morphology we augment our sample with data of spiral and elliptical galaxies from the literature , in which old GCs are reliably detected . This large dataset confirms ( irrespective of galaxy type ) the increase of the specific frequencies of GCs above and below a galaxy magnitude of M _ { V } \simeq - 20 mag . Over the full mass range , the S _ { L } - value of early-type galaxies is , on average , twice that of late-types . To investigate the observed trends we derive theoretical predictions of GC system scaling parameters as a function of host galaxy mass based on the models of ( ) in which star-formation processes are regulated by stellar and supernova feedback below a stellar mass of 3 \times 10 ^ { 10 } { \cal M } _ { \odot } , and by virial shocks above it . We find that the analytical model describes remarkably well the shape of the GC system scaling parameter distributions with a universal specific GC formation efficiency , \eta , which relates the total mass in GCs to the total galaxy halo mass . Early-type and late-type galaxies show a similar mean value of \eta = 5.5 \times 10 ^ { -5 } , with an increasing scatter towards lower galaxy masses . This can be due to the enhanced stochastic nature of the star and star-cluster formation processes for such systems . Some massive galaxies have excess \eta values compared to what is expected from the mean model prediction for galaxies more luminous than M _ { V } \simeq - 20 mag ( L _ { V } \gtrsim 10 ^ { 10 } L _ { \odot } ) . This may be attributed to a very efficient early GC formation , less efficient production of field stars or accretion of predominantly low-mass/luminosity high - \eta galaxies , or a mixture of all these effects .