  Early dark energy (EDE) offers a solution to the so-called Hubble tension.
Recently, it was shown that the constraints on EDE using Markov Chain Monte
Carlo are affected by prior volume effects. The goal of this paper is to
present constraints on the fraction of EDE, $f_\mathrm{EDE}$, and the Hubble
parameter, $H_0$, which are not subject to prior volume effects. We conduct a
frequentist profile likelihood analysis considering Planck cosmic microwave
background, BOSS full-shape galaxy clustering, DES weak lensing, and SH0ES
supernova data. Contrary to previous findings, we find that $H_0$ for the EDE
model is in statistical agreement with the SH0ES direct measurement at $\leq
1.7\,\sigma$ for all data sets. For our baseline data set (Planck + BOSS), we
obtain $f_\mathrm{EDE} = 0.087\pm 0.037$ and $H_0 = 70.57 \pm 1.36\,
\mathrm{km/s/Mpc}$ at $68\%$ confidence limit. We conclude that EDE is a viable
solution to the Hubble tension.
