  We study the validity of inspiral templates in gravitational wave data
analysis with Advanced LIGO sensitivity for low mass binary black holes with
total masses of $M \leq 30 Msun$. We mainly focus on the nonspinning system. As
our complete inspiral-merger-ringdown waveform model ($IMR$), we assume the
phenomenological model, "PhenomA", and define our inspiral template model
($Imerg$) by taking the inspiral part into account from $IMR$ up to the merger
frequency (fmerg). We first calculate the {\it true} statistical uncertainties
using $IMR$ signals and $IMR$ templates. Next, using $IMR$ signals and $Imerg$
templates, we calculate fitting factors and systematic biases, and compare the
biases with the {\it true} statistical uncertainties. We find that the valid
criteria of the bank of $Imerg$ templates are obtained as $Mcrit \sim 24 Msun$
for detection (if $M>Mcrit$, the fitting factor is smaller than $0.97$), and
$Mcrit \sim 26 Msun$ for parameter estimation (if $M>Mcrit$, the systematic
bias is larger than the {\it true} statistical uncertainty where the signal to
noise ratio is $20$), respectively. In order to see the dependence on the
cutoff frequency of the inspiral waveforms, we define another inspiral model
$Iisco$ which is terminated at the innermost-stable-circular-orbit frequency
($fisco<fmerg$). We find that the valid criteria of the bank of $Iisco$
templates are obtained as $Mcrit \sim 15 Msun$ and $\sim 17 Msun$ for detection
and parameter estimation, respectively. We investigate the statistical
uncertainties for the inspiral template models considering various signal to
noise ratios, and compare those to the {\it true} statistical uncertainties. We
also consider the aligned-spinning system with fixed mass ratio ($m_1/m_2=3$)
and spin ($\chi=0.5$) by employing the recent phenomenological model,
"PhenomC".
