  LS V +44 17 is a persistent Be/X-ray binary (BeXRB) that displayed a bright,
double-peaked period of X-ray activity in late 2022/early 2023. We present a
radio monitoring campaign of this outburst using the Very Large Array. Radio
emission was detected, but only during the second, X-ray brightest, peak, where
the radio emission followed the rise and decay of the X-ray outburst. LS V +44
17 is therefore the third neutron star BeXRB with a radio counterpart. Similar
to the other two systems (Swift J0243.6+6124 and 1A 0535+262), its X-ray and
radio luminosity are correlated: we measure a power law slope $\beta =
1.25^{+0.64}_{-0.30}$ and a radio luminosity of $L_R =
(1.6\pm0.2)\times10^{26}$ erg/s at a $0.5-10$ keV X-ray luminosity of
$2\times10^{36}$ erg/s (i.e. $\sim 1\%$ $L_{\rm Edd}$). This correlation index
is slightly steeper than measured for the other two sources, while its radio
luminosity is higher. We discuss the origin of the radio emission, specifically
in the context of jet launching. The enhanced radio brightness compared to the
other two BeXRBs is the first evidence of scatter in the giant BeXRB outburst
X-ray--radio correlation, similar to the scatter observed in sub-classes of
low-mass X-ray binaries. While a universal explanation for such scatter is not
known, we explore several options: we conclude that the three sources do not
follow proposed scalings between jet power and neutron star spin or magnetic
field, and instead briefly explore the effects that ambient stellar wind
density may have on BeXRB jet luminosity.
