  Coalescing binary black holes (BBHs) are among the most likely sources for
the Laser Interferometer Gravitational-wave Observatory (LIGO) and its
international partners Virgo and KAGRA. Optimal searches for BBHs require
accurate waveforms for the signal model and effectual template banks that cover
the mass space of interest. We investigate the ability of the second-order
post-Newtonian TaylorF2 hexagonal template placement metric to construct an
effectual template bank, if the template waveforms used are effective one body
waveforms tuned to numerical relativity (EOBNRv2). We find that by combining
the existing TaylorF2 placement metric with EOBNRv2 waveforms, we can construct
an effectual search for BBHs with component masses in the range 3 Msolar <=
m_1, m_2 <= 25 Msolar. We also show that the (computationally less expensive)
TaylorF2 post-Newtonian waveforms can be used in place of EOBNRv2 waveforms
when M <~ 11.4 Msolar. Finally, we investigate the effect of modes other than
the dominant l = m = 2 mode in BBH searches. We find that for systems with
(m_1/m_2)<= 1.68 or inclination angle: \iota <= 0.31 or \iota >= 2.68 radians,
there is no significant loss in the total possible signal-to-noise ratio due to
neglecting modes other than l = m = 2 in the template waveforms. For a source
population uniformly distributed in spacial volume, over the entire sampled
region of the component-mass space, the loss in detection rate (averaged over a
uniform distribution of inclination angle and sky-location/polarization
angles), remains below ~11%. For binaries with high mass-ratios \textit{and}
0.31 <= \iota <= 2.68, including higher order modes could increase the
signal-to-noise ratio by as much as 8% in Advanced LIGO. Our results can be
used to construct matched-filter searches in Advanced LIGO and Advanced Virgo.
