This applies to FLRW models, which LCDM is based on.
FLRW models have a Hubble parameter, $H$, and a Hubble constant, $H_0$, related by this:
$$H = H_0 [\Omega_M (1+z)^3 + \Omega_\Lambda]^{1/2}$$
Hubble’s constant, $H_0$ is the expansion rate today.
In a de Sitter model, aka pure dark energy, aka exponentially expanding model you have:
$$\Omega_M = 0.0$$
$$\Omega_\Lambda = 1.0$$
$$[\Omega_M (1+z)^3 + \Omega_\Lambda] = 1$$
$$H = H_0$$
The expansion rate never changes.
In LCDM you have:
$$\Omega_M = 0.3$$
$$\Omega_\Lambda = 0.7$$
Which gives us something like this:
It was larger in the past, and is settles on a value around 55 in the infinite future.
You can use this to try your own parameters:
https://mikehelland.github.io/hubbles-law/other/expansionrate/expansionrate.htm
To try to address a question by @ExpEarth, you can play with the parameters like this:
$$\Omega_M = -0.1$$
$$\Omega_\Lambda = 1.1$$
And the Hubble parameter will be lower in the past, rather than higher. I tried to compute luminosity distances that model, but it started complaining about not real numbers.
As is explained in the section Hubble Parameter at my website, the favorite model associated with the Variable Mass Theory is a de Sitter like cosmological model with accompanying constant Hubble parameter and an ( equivalent ) exponential expansion rate that never changes. A non-empty universe, filled with common mass and without dark energy.