  In preparation for the Jan 1/2019 encounter between the New Horizons
spacecraft and the Kuiper Belt object 2014 MU69, we provide estimates of the
expected impact crater surface density on the Kuiper Belt object. Using the
observed crater fields on Charon and Pluto down to the resolution limit of the
2015 New Horizons flyby of those bodies and estimates of the orbital
distribution of the crater-forming projectiles, we calculate the number of
craters per unit area formed as a function of the time a surface on 2014 MU69
has been exposed to bombardment. We find that if the shallow crater-size
distribution from 1-15 km exhibited on Pluto and Charon is indeed due to the
sizes of Kuiper Belt projectiles, 2014 MU69 should exhibit a surface that is
only lightly cratered below 1 km scale, despite being bombarded for
$\sim4$~billion years. Its surface should therefore be more clearly indicative
of its accretionary environment. In addition, this object may the first
observed for which the majority of the bombardment is from exogenic projectiles
moving less than or near the speed of sound in the target materials, implying
morphologies more akin to secondary craters elsewhere in the Solar System.
Lastly, if the shallow Kuiper Belt size distribution implied from the Pluto and
Charon imaging is confirmed at MU69, then we conclude that this size
distribution is a preserved relic of its state $\simeq$4.5~Gyr ago and provides
a direct constraint on the planetesimal formation process itself.
