  We present a systematic survey the range of predictions of the neutron star
inner crust composition, crust-core transition densities and pressures, and
density range of the nuclear `pasta' phases at the bottom of the crust provided
by the compressible liquid drop model in the light of current experimental and
theoretical constraints on model parameters. Using a Skyrme-like model for
nuclear matter, we construct baseline sequences of crust models by consistently
varying the density dependence of the bulk symmetry energy at nuclear
saturation density, $L$, under two conditions: (i) that the magnitude of the
symmetry energy at saturation density $J$ is held constant, and (ii) $J$
correlates with $L$ under the constraint that the pure neutron matter (PNM) EoS
satisfies the results of ab-initio calculations at low densities. Such baseline
crust models facilitate consistent exploration of the $L$ dependence of crustal
properties. The remaining surface energy and symmetric nuclear matter
parameters are systematically varied around the baseline, and different
functional forms of the PNM EoS at sub-saturation densities implemented, to
estimate theoretical `error bars' for the baseline predictions. Inner crust
composition and transition densities are shown to be most sensitive to the
surface energy at very low proton fractions and to the behavior of the
sub-saturation PNM EoS. Recent calculations of the energies of neutron drops
suggest that the low-proton-fraction surface energy might be higher than
predicted in Skyrme-like models, which our study suggests may result in a
greatly reduced volume of pasta in the crust than conventionally predicted.
