  We present the analysis of the binary-lens microlensing event
OGLE-2017-BLG-0537. The light curve of the event exhibits two strong
caustic-crossing spikes among which the second caustic crossing was resolved by
high-cadence surveys. It is found that the lens components with a mass ratio
$\sim 0.5$ are separated in projection by $\sim 1.3\thetae$, where $\thetae$ is
the angular Einstein radius. Analysis of the caustic-crossing part yields
$\thetae=1.77\pm 0.16$~mas and a lens-source relative proper motion of $\mu
=12.4\pm 1.1~{\rm mas}~{\rm yr}^{-1}$. The measured $\mu$ is the third highest
value among the events with measured proper motions and $\sim 3$ times higher
than the value of typical Galactic bulge events, making the event a strong
candidate for follow-up observations to directly image the lens by separating
it from the source. From the angular Einstein radius combined with the
microlens parallax, it is estimated that the lens is composed of two
main-sequence stars with masses $M_1\sim 0.4~M_\odot$ and $M_2\sim 0.2~M_\odot$
located at a distance of $D_{\rm L}\sim 1.2$~kpc. However, the physical lens
parameters are not very secure due to the weak microlens-parallax signal, and
thus we cross check the parameters by conducting a Bayesian analysis based on
the measured Einstein radius and event timescale combined with the blending
constraint. From this, we find that the physical parameters estimated from the
Bayesian analysis are consistent with those based on the measured microlens
parallax. Resolving the lens from the source can be done in about 5 years from
high-resolution follow-up observations and this will provide a rare opportunity
to test and refine the microlensing model.
