  We explore the relative strength of the narrow emission lines in an SDSS
based sample of broad H-alpha selected AGN, defined in paper I. We find a
decrease in the narrow to broad H-alpha luminosity (L_bHa) ratio with
increasing L_bHa, such that both L([OIII] lambda5007) and L(narrow H-alpha)
scale as L_bHa^0.7 for 10^40 < L_bHa < 10^45 ergs s^-1. Following our earlier
result that L_bHa \propto L_bol, this trend indicates that the relative narrow
line luminosity decreases with increasing L_bol. We derive L_bol / 10^43 ergs
s^-1 = 4000 (L([OIII]) / 10^43 ergs s^-1)^1.39. This implies that the
bolometric correction factor, L_bol / L([OIII]), decreases from 3,000 at L_bol
= 10^46.1 ergs s^-1 to 300 at L_bol = 10^42.5 ergs s^-1. At low luminosity, the
narrow component dominates the observed H-alpha profile, and most type 1 AGN
appear as intermediate type AGN. Partial obscuration or extinction cannot
explain the dominance of intermediate type AGN at low luminosity, and the most
likely mechanism is a decrease in the narrow line region covering factor with
increasing L_bol. Deviations from the above trend occur in objects with L /
L_Edd <~ 10^-2.6, probably due to the transition to LINERs with suppressed
[OIII] emission, and in objects with M_BH > 10^8.5 M_Sun, probably due to the
dominance of radio loud AGN, and associated enhanced [OIII] emission.
