Interpretation of horizon in de Sitter

Given the de Sitter metric for spacetime
$$ds^2 = left( 1 – frac{Lambda}{3}r^2right) dt^2 – frac{1}{left( 1 – frac{Lambda}{3}r^2 right)}dr^2 – r^2dOmega^2 $$
we understand this is a solution to Einstein’s field equations in vacuum with the addition of a cosmological constant which is maximally symmetric. In this static coordinates there is an apparent issue at $r=sqrt{3/Lambda}$, where the metric becomes singular. My question is (staying within this coordinates) how can I interpret this singularity?

It seems like a horizon since beyond that point the signs in front of the $t$ and the $r$ coordinate are switched. But how can I make sense of this under the context of an expanding universe. I guess things that are found at a coordinate $r>sqrt{3/Lambda}$ are receding from the observer faster than light and are therefore casually disconnected. But what about something from beyond this horizon, falling in… I suppose the answer is that to travel into the $r<sqrt{3/Lambda}$ region they would need to go faster than light and thus nothing happens.

EDIT

I think the horizon issue is clear for geodesics and point particles. But let us consider for example a scalar field, which is supposed to be continuous and differentiable (twice at least) which is supposed to be defined everywhere. Any differential equation for it will, have trouble at the horizon. I am not sure how to handle the two regions. Should I expect a discontinuity in the field or something of that sort?