  To understand better the early galactic production of Li, Be, and B by cosmic
ray spallation and fusion reactions, the dependence of these production rates
on cosmic ray models and model parameters is examined. The sensitivity of
elemental and isotopic production to the cosmic ray pathlength magnitude and
energy dependence, source spectrum, spallation kinematics, and cross section
uncertainties is studied. Changes in these model features, particularly those
features related to confinement, are shown to alter the Be- and B-versus-Fe
slopes {}from a na\"{\i}ve quadratic relation. The implications of our results
for the diffuse $\gamma$-ray background are examined, and the role of chemical
evolution and its relation to our results is noted. It is also noted that the
unmeasured high energy behavior of $\alpha+\alpha$ fusion can lead to effects
as large as a factor of 2 in the resultant yields. Future data should enable
Population II Li, Be, and B abundances to constrain cosmic ray models for the
early Galaxy.
