  We have tabulated lists of upper red giant, horizontal, and asymptotic giant
branch (RGB, HB, AGB) stars in the globular cluster M5 that are complete to
over 10' from the core for the RGB and AGB samples, and 8' for the HB sample.
The large samples give us the most precise value of R_2 = N_AGB / N_HB to date
for a single globular cluster (0.176 +/- 0.018). This is incompatible with
theoretical calculations using the most recent physical inputs. The discrepancy
can probably be attributed to the dependence of observed R_2 values on
horizontal branch morphology. We identify the cluster M55 as being another
possible example of this effect. Samples of HB and AGB stars in populous
clusters may provide a means of calibrating the masses of horizontal branch
stars in globular clusters. The cumulative luminosity function of the upper red
giant branch shows an apparent deficit of observed stars near the tip of the
branch. This feature has less than a 2% chance of being due to statistical
fluctuations. The slope of the cumulative luminosity function for AGB stars is
consistent with the theoretically predicted value from stellar models when
measurement bias is taken into account. We also introduce a new diagnostic
R_clump that reflects the fraction of the AGB lifetime that a star spends in
the AGB clump. For M5, we find R_clump = 0.42 +/- 0.05, in marginal
disagreement with theoretical predictions. Finally, we note that the blue half
of M5's instability strip (where first overtone RR Lyraes reside) is
underpopulated, based on the large numbers of fundamental mode RR Lyraes and on
the nonvariable stars at the blue end of the instability strip. This fact may
imply that the evolutionary tracks (and particularly the colors) of stars in
the instability strip are affected by pulsations.
