  We study the effectiveness of stationary-phase approximated post-Newtonian
waveforms currently used by ground-based gravitational-wave detectors to search
for the coalescence of binary black holes by comparing them to an accurate
waveform obtained from numerical simulation of an equal-mass non-spinning
binary black hole inspiral, merger and ringdown. We perform this study for the
Initial- and Advanced-LIGO detectors. We find that overlaps between the
templates and signal can be improved by integrating the match filter to higher
frequencies than used currently. We propose simple analytic frequency cutoffs
for both Initial and Advanced LIGO, which achieve nearly optimal matches, and
can easily be extended to unequal-mass, spinning systems. We also find that
templates that include terms in the phase evolution up to 3.5 pN order are
nearly always better, and rarely significantly worse, than 2.0 pN templates
currently in use. For Initial LIGO we recommend a strategy using templates that
include a recently introduced pseudo-4.0 pN term in the low-mass ($M \leq 35
\MSun$) region, and 3.5 pN templates allowing unphysical values of the
symmetric reduced mass $\eta$ above this. This strategy always achieves
overlaps within 0.3% of the optimum, for the data used here. For Advanced LIGO
we recommend a strategy using 3.5 pN templates up to $M=12 \MSun$, 2.0 pN
templates up to $M=21 \MSun$, pseudo-4.0 pN templates up to $65 \MSun$, and 3.5
pN templates with unphysical $\eta$ for higher masses. This strategy always
achieves overlaps within 0.7% of the optimum for Advanced LIGO.
