  We introduce a new method for measuring the Hubble parameter from
low-redshift large-scale observations that is independent of the comoving sound
horizon. The method uses the baryon-to-photon ratio determined by the
primordial deuterium abundance, together with Big Bang Nucleosynthesis (BBN)
calculations and the present-day CMB temperature to determine the physical
baryon density $\Omega_b h^2$. The baryon fraction $\Omega_b/\Omega_m$ is
measured using the relative amplitude of the baryonic signature in galaxy
clustering measured by the Baryon Oscillation Spectroscopic Survey, scaling the
physical baryon density to the physical matter density. The physical density
$\Omega_mh^2$ is then compared with the geometrical density $\Omega_m$ from
Alcock-Paczynski measurements from Baryon Acoustic Oscillations (BAO) and
voids, to give $H_0$. Including type Ia supernovae and uncalibrated BAO, we
measure $H_0 = 67.1^{+6.3}_{-5.3}$ km s$^{-1}$ Mpc$^{-1}$. We find similar
results when varying analysis choices, such as measuring the baryon signature
from the reconstructed correlation function, or excluding supernovae or voids.
This measurement is currently consistent with both the distance-ladder and CMB
$H_0$ determinations, but near-future large-scale structure surveys will obtain
3--4$\times$ tighter constraints.
