  We present a reduced-order surrogate model of gravitational waveforms from
non-spinning binary black hole systems with comparable to large mass-ratio
configurations. This surrogate model, \texttt{BHPTNRSur1dq1e4}, is trained on
waveform data generated by point-particle black hole perturbation theory
(ppBHPT) with mass ratios varying from 2.5 to 10,000. \texttt{BHPTNRSur1dq1e4}
extends an earlier waveform model, \texttt{EMRISur1dq1e4}, by using an updated
transition-to-plunge model, covering longer durations up to 30,500 $m_1$ (where
$m_1$ is the mass of the primary black hole), includes several more spherical
harmonic modes up to $\ell=10$, and calibrates subdominant modes to numerical
relativity (NR) data. In the comparable mass-ratio regime, including mass
ratios as low as $2.5$, the gravitational waveforms generated through ppBHPT
agree surprisingly well with those from NR after this simple calibration step.
We also compare our model to recent SXS and RIT NR simulations at mass ratios
ranging from $15$ to $32$, and find the dominant quadrupolar modes agree to
better than $\approx 10^{-3}$. We expect our model to be useful to study
intermediate-mass-ratio binary systems in current and future gravitational-wave
detectors.
