= Solution
Increasing the <dark energy> density makes dark-energy domination begin earlier. The larger <Hubble parameter> strengthens the $2H\dot\Delta_m$ friction term while the clustering source $4\pi G\bar\rho_m\Delta_m$ continues to dilute, so less <large-scale structure of the universe> can grow from a fixed primordial amplitude.
Deep in cosmological-constant domination, $H\simeq H_\Lambda$ is constant and $\bar\rho_m$ is negligible. The growth equation reduces to
$$
\ddot\Delta_m+2H_\Lambda\dot\Delta_m=0,
$$
and hence
$$
\boxed{\Delta_m=C_1+C_2e^{-2H_\Lambda t}
=C_1+C_2a^{-2}}.
$$
The surviving mode is constant: \b[matter growth freezes].
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