  We develop a model for frequency-domain gravitational waveforms from
inspiraling binary neutron stars. Our waveform model is calibrated by
comparison with hybrid waveforms constructed from our latest high-precision
numerical-relativity waveforms and the SEOBNRv2T waveforms in the frequency
range of $10$--$1000\,{\rm Hz}$. We show that the phase difference between our
waveform model and the hybrid waveforms is always smaller than $0.1\, {\rm
rad}$ for the binary tidal deformability, ${\tilde \Lambda}$, in the range
$300\lesssim{\tilde \Lambda}\lesssim1900$ and for the mass ratio between 0.73
and 1. We show that, for $10$--$1000\,{\rm Hz}$, the distinguishability for the
signal-to-noise ratio $\lesssim50$ and the mismatch between our waveform model
and the hybrid waveforms are always smaller than 0.25 and $1.1\times10^{-5}$,
respectively. The systematic error of our waveform model in the measurement of
${\tilde \Lambda}$ is always smaller than $20$ with respect to the hybrid
waveforms for $300\lesssim{\tilde \Lambda}\lesssim1900$. The statistical error
in the measurement of binary parameters is computed employing our waveform
model, and we obtain results consistent with the previous studies. We show that
the systematic error of our waveform model is always smaller than $20\%$
(typically smaller than $10\%$) of the statistical error for events with the
signal-to-noise ratio of $50$.
