A 5% measurement of the Hubble constant from Type II supernovae
  The most stringent local measurement of the Hubble constant from
Cepheid-calibrated Type Ia supernovae (SNe~Ia) differs from the value inferred
via the cosmic microwave background radiation ({\it Planck}$+\Lambda$CDM) by
more than 5$\sigma$. This so-called "Hubble tension" has been confirmed by
other independent methods, and thus does not appear to be a possible
consequence of systematic errors. Here, we continue upon our prior work of
using Type II supernovae to provide another, largely-independent method to
measure the Hubble constant. From 13 SNe~II with geometric, Cepheid, or tip of
the red giant branch (TRGB) host-galaxy distance measurements, we derive H$_0=
75.4^{+3.8}_{-3.7}$ km s$^{-1}$ Mpc$^{-1}$ (statistical errors only),
consistent with the local measurement but in disagreement by $\sim 2.0\sigma$
with the Planck $+\Lambda$CDM value. Using only Cepheids ($N=7$), we find H$_0
= 77.6^{+5.2}_{-4.8}$ km s$^{-1}$ Mpc$^{-1}$, while using only TRGB ($N=5$), we
derive H$_0 = 73.1^{+5.7}_{-5.3}$ km s$^{-1}$ Mpc$^{-1}$. Via 13 variants of
our dataset, we derive a systematic uncertainty estimate of 1.5 km s$^{-1}$
Mpc$^{-1}$. The median value derived from these variants differs by just 0.3 km
s$^{-1}$ Mpc$^{-1}$ from that produced by our fiducial model. Because we only
replace SNe~Ia with SNe~II -- and we do not find tension between the Cepheid
and TRGB H$_0$ measurements -- our work reveals no indication that SNe~Ia or
Cepheids could be the sources of the "H$_0$ tension." We caution, however, that
our conclusions rest upon a modest calibrator sample; as this sample grows in
the future, our results should be verified.
