  Recent studies have highlighted the sensitivity of core-collapse supernovae
(CCSNe) models to electron-capture (EC) rates on neutron-rich nuclei near the
N=50 closed-shell region. In this work, we perform a large suite of
one-dimensional CCSN simulations for 200 stellar progenitors using recently
updated EC rates in this region. For comparison, we repeat the simulations
using two previous implementations of EC rates: a microphysical library with
parameterized N=50 rates (LMP), and an older independent-particle approximation
(IPA). We follow the simulations through shock revival up to several seconds
post-bounce, and show that the EC rates produce a consistent imprint on CCSN
properties, often surpassing the role of the progenitor itself. Notable impacts
include the timescale of core collapse, the electron fraction and mass of the
inner core at bounce, the accretion rate through the shock, the success or
failure of revival, and the properties of the central compact remnant. We also
compare the observable neutrino signal of the neutronization burst in a
DUNE-like detector, and find consistent impacts on the counts and mean
energies. Overall, the updated rates result in properties that are intermediate
between LMP and IPA, and yet slightly more favorable to explosion than both.
