  We present \textit{ALMA} 1.3 mm and 0.86 mm observations of the nearby (17.34
pc) F9V star q1 Eri (HD 10647, HR 506). This system, with age ${\sim}1.4$ Gyr,
hosts a ${\sim}2$ au radial velocity planet and a debris disc with the highest
fractional luminosity of the closest 300 FGK type stars. The \textit{ALMA}
images, with resolution ${\sim}0.5''$, reveal a broad (34{-}134 au) belt of
millimeter emission inclined by $76.7{\pm}1.0$ degrees with maximum brightness
at $81.6{\pm}0.5$ au. The images reveal an asymmetry, with higher flux near the
southwest ansa, which is also closer to the star. Scattered light observed with
the Hubble Space Telescope is also asymmetric, being more radially extended to
the northeast. We fit the millimeter emission with parametric models and place
constraints on the disc morphology, radius, width, dust mass, and scale height.
We find the southwest ansa asymmetry is best fitted by an extended clump on the
inner edge of the disc, consistent with perturbations from a planet with mass
$8 M_{\oplus} {-} 11 M_{\rm Jup}$ at ${\sim}60$ au that may have migrated
outwards, similar to Neptune in our Solar System. If the measured vertical
aspect ratio of $h{=}0.04{\pm}0.01$ is due to dynamical interactions in the
disc, then this requires perturbers with sizes ${>}1200$ km. We find tentative
evidence for an 0.86 mm excess within 10 au, $70{\pm}22\, \mu$Jy, that may be
due to an inner planetesimal belt. We find no evidence for CO gas, but set an
upper bound on the CO gas mass of $4{\times}10^{-6}$ M$_{\oplus}$
($3\,\sigma$), consistent with cometary abundances in the Solar System.
