  Type Ibn supernovae (SNe Ibn) are rare stellar explosions powered primarily
by interaction between the SN ejecta and H-poor, He-rich material lost by their
progenitor stars. Multi-wavelength observations, particularly in the X-rays, of
SNe Ibn constrain their poorly-understood progenitor channels and mass-loss
mechanisms. Here we present Swift X-ray, ultraviolet, and ground-based optical
observations of the Type Ibn SN 2022ablq -- only the second SN Ibn with X-ray
detections to date. While similar to the prototypical Type Ibn SN 2006jc in the
optical, SN 2022ablq is roughly an order of magnitude more luminous in the
X-rays, reaching unabsorbed luminosities $L_X$ $\sim$ 3$\times$10$^{40}$ erg
s$^{-1}$ between 0.2 - 10 keV. From these X-ray observations we infer
time-varying mass-loss rates between 0.05 - 0.5 $M_\odot$ yr$^{-1}$ peaking 0.5
- 2 yr before explosion. This complex mass-loss history and circumstellar
environment disfavor steady-state winds as the primary progenitor mass-loss
mechanism. We also search for precursor emission from alternative mass-loss
mechanisms, such as eruptive outbursts, in forced photometry during the two
years before explosion. We find no statistically significant detections
brighter than M $\approx$ -14 -- too shallow to rule out precursor events
similar to those observed for other SNe Ibn. Finally, numerical models of the
explosion of a $\sim$15 $M_\odot$ helium star that undergoes an eruptive
outburst $\approx$1.8 years before explosion are consistent with the observed
bolometric light curve. We conclude that our observations disfavor a Wolf-Rayet
star progenitor losing He-rich material via stellar winds and instead favor
lower-mass progenitor models, including Roche-lobe overflow in helium stars
with compact binary companions or stars that undergo eruptive outbursts during
late-stage nucleosynthesis stages.
