Can weak gravitational lensing or microlensing-induced wavefront distortion limit resolution of absurdly large aperture telescopes? This is a theoretical question. 

This answer to the question If we had the right technology could we see a distant star in detail? (presumably space-based) primarily addresses the scaling of diffraction-limited resolution with aperture $D$. For existing and near-future telescopes this is assumed to follow $\lambda/D$.

Imagine a future optical or radio interferometric telescope of absurdly large effective aperture or baseline, say AU or even larger, operated similarly to the Event Horizon Telescope (local downconversion and timestamping, interferometry performed offline)

Could weak gravitational lensing effects or gravitational microlensing result in wavefront distortion that if not corrected, would result in degraded resolution? Note I'm not asking about distortion of the field, but instead a limitation to the resolution; degraded point spread function.

If so, would this problem be amenable to correction in the same way that atmospheric and ionospheric effects (visible and radio) are dealt with? Would it generally be static on the timescale of the observation?
As far as microlensing is concerned:

Not likely

This is a bit of a dodge on the question, but it is hard to come up with a scenario where microlensing becomes the dominant PSF term. 

Microlensing occurs during conjunction with a stellar or planetary object, and results in a momentary (seconds-to-days timescale) increase in the brightness of the observed star. It is an extremely rare event, with rates around 100 in 17 million stars in the most recent surveys.

Stellar densities ($\rho$) around our solar system are on the order of 0.14 stars per cubic parsec. With such a low number density, microlensing does not pose any practical limitation on the resolution of radio telescopes. Lets do some scratch-pad estimates to see:

If we assume a synthetic aperture ($D$) of 1AU ($4.84\times10^{-6}$parsecs) , a wavelength ($\lambda$) of 1mm (similar to the view of Betelguese by the ALMA observatory) , and a desired spatial resolution ($s$) of 10,000 km at a distance $L$:

$$
\begin{align}
\frac{s}{L}  &amp;= 1.22 \frac{\lambda }{D} \\
L &amp;= \frac{sD}{1.22 \lambda } = 40\;\text{kilo-parsec}
\end{align}
$$

This is roughly the diameter of the milky way galaxy. So an interferometer operating in the 1mm wavelength with a 1AU baseline has a 10,000 km resolution at a distance of 40 kpc.  

How many stars are between the 1AU-wide observatory and the target star? Using a cone of base diameter $D$ and height $L$ as a volume and the above stellar density, we get the average number of stars ($N$) between our aperture and the observed star:
$$ N = \rho \frac{\pi}{12}D^2 L = 3 \times 10^{-8} \; \text{stars}$$

You would have to ramp $D$ up by a factor of $10^4$ before $N \approx 1$ and 'microlensing aberrations' were more than just an extremely rare event.